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Table 2
Systems where a single planet would have to be more massive than 0id=MJup to sculpt the disc inner edge (to 1σ)
| System | Mp (Mjup) | Qp (arcsec) | Mp,n (Mjup) | Mp,stir (Mjup) | Mdísc,stír (M?) | M. (M?) | t* (Myr) | idisc(°) |
|---|---|---|---|---|---|---|---|---|
| HD 138813 | 2.8 ± 0.5 |  |
0.4 ± 0.2 | 3±2 | 4000 ± 1000 |  |
10±3 |  |
| HD 218396 |  |
 |
 |
 |
5000 ± 1000 | 1.59 ± 0.02 |  |
31 ± 3 |
| HD 38206 | 2.3 ± 0.3 | 1.5 ± 0.3 |  |
0.08 ± 0.09 |  |
2.36 ± 0.02 |  |
83 ± 1 |
| HD 146897 | 2.0 ± 0.4 |  |
 |
0.06 ± 0.07 | 1000 ± 500 | 1.32 ± 0.03 | 10±3 | 89±5 |
| HD 121617 | 1.9 ± 0.3 | 0.32 ± 0.04 | 0.19 ± 0.06 | 0.3 ± 0.2 | 900 ± 200 |  |
16±3 |  |
| HD 146181 |  |
 |
 |
0.04 ± 0.05 |  |
 |
16±2 | 79 ± 7 |
| HD 181327 | 1.6 ± 0.1 | 1.120 ± 0 009 | 0 20 ± 0 03 | 0.024 ± 0.008 | 750 ± 70 | 1.41 ± 0.02 | 24±3 | 30.0 ± 0.5 |
| HD 131835 | 1.6 ± 0.1 | 0.23 ± 0.01 | 0.13 ± 0.02 | 1.2 ± 0.5 | 1500±100 |  |
16±2 | 73.7 ± 0.4 |
| HD 111520 | 1.5 ± 0.3 |  |
 |
0.2 ± 0.2 | 1000 ± 400 |  |
15±3 |  |
| HD 21997 |  |
0.74 ± 0.04 | 0.11 ± 0.02 | 0.07 ± 0.03 |  |
1.83 ± 0.02 |  |
 |
| HD 9672 | 1.4 ± 0.1 |  |
0.10 ± 0.02 |  |
2300 ± 200 | 1.98 ± 0.01 | 45 ± 5 | 79.1 ± 0.4 |
| HD 188228 | 1.2 ± 0.6 | 1.0± 0 7 | 0.06 ± 0.07 | 1±3 | 100 ± 100 | 2.34 ± 0.02 | 45 ± 5 | 50 ± 20 |
| HD 121191 | 1.1 ± 0.2 | 0.16 ± 0.04 | 0.08 ± 0.03 | 0.5 ± 0.4 |  |
 |
16±3 |  |
| CPD-72 2713 |  |
 |
 |
 |
6000 ± 3000 | 0.80 ± 0.02 | 24±3 |  |
| HD 191089 |  |
0.56 ± 0.03 | 0 06 ± 0 01 | 0.017 ± 0.006 | 110±10 |  |
24 ± 3 | 60 ± 1 |
| HD 15115 | 0 85 ± 0 09 | 0.70 ± 0.09 | 0.05 ± 0.01 | 0.07 ± 0.04 | 290 ± 30 | 1.40 ± 0.02 | 45 ± 4 | 86.2 ± 0.5 |
| HD 61005 |  |
1.12 ± 0.02 | 0.053 ± 0.008 | 0.03 ± 0.01 |  |
 |
45 ± 5 | 85.7 ± 0.2 |
| HD 192425 | 0.7 ± 0.2 | 1.6 ± 0.5 | 0.02 ± 0.01 | 0.8 ± 1.0 | 1500±700 | 1.94 ± 0.04 | 400 ± 100 | 71 ± 5 |
Notes. These systems would make good targets for future planet searches. The best targets require high planet masses to sculpt and stir the discs (Mp, Mp,n, Mp,stìr), require planet orbits that are well-separated from the star at their maximum elongation (Qp), would require potentially unfeasible disc masses to self stir (Mdisc,stir), are young (t*), and whose discs have low sky-plane inclinations (idisc). The systems are ordered by the mass of the single planet required to sculpt the disc inner edge, Mp. Only systems with resolved discs are shown; all are resolved by ALMA except HD 188228 and HD 192425, which are resolved by Herschel. Uncertainties are 1σ.
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